The role of ejecta in the small crater populations on the mid-sized saturnian satellites

Bierhaus, E. B.; Dones, L.; Alvarellos, J. L.; Zahnle, Kevin

doi:10.1016/j.icarus.2011.12.011

Cited by 53 publications

(73 citation statements)

References 62 publications

(92 reference statements)

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“…Hence, it is possible that the locations of these impacts are outside the mapped area in the northern hemisphere. This would be consistent with the prediction that on a low gravity body the secondary craters form far away from the parent primary (e.g., Bierhaus et al, 2012). Another possible origin of these features might be related to fractures.…”

Section: Geologic Mapsupporting

confidence: 89%

“…Because it is not always possible to discriminate between a primary crater from a self-secondary crater, the derived age on ejecta blanket can be considered as a maximum age. This effect, however, might be less important for Vesta since it has been predicted that secondary craters on Vesta would form far away from the source crater (e.g., Bierhaus et al, 2012;Schmedemann et al, in preparation). We avoided counting on potential impact melt deposits (e.g., Williams et al, in press) because for such surfaces the target properties influence the diameter of craters formed in the strength regime (e.g., Dundas et al, 2010;van der Bogert et al, 2010van der Bogert et al, , 2013.…”

Section: Datasets and Methodsmentioning

confidence: 99%

“…Furrows found within the ejecta blanket or close to the crater could be formed by material ejected at a high angle from the source crater (i.e., >45°). The high ejection angle would have prevented the material moving far away from the crater and create secondary craters outside the ejecta blanket (Schmedemann et al, in preparation; Bierhaus et al, 2012). Krohn et al (2013) mapped the distribution of the asymmetric craters on a global scale and discussed their formation on Vesta.…”

Section: This Issue)mentioning

confidence: 99%

See 2 more Smart Citations

Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Ruesch

Hiesinger

Blewett

et al. 2014

Icarus

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a b s t r a c tThe Dawn Framing Camera (FC) has imaged the northern hemisphere of the Asteroid (4) Vesta at high spatial resolution and coverage. This study represents the first investigation of the overall geology of the northern hemisphere (22-90°N, quadrangles Av-1, 2, 3, 4 and 5) using these unique Dawn mission observations. We have compiled a morphologic map and performed crater size-frequency distribution (CSFD) measurements to date the geologic units. The hemisphere is characterized by a heavily cratered surface with a few highly subdued basins up to $200 km in diameter. The most widespread unit is a plateau (cratered highland unit), similar to, although of lower elevation than the equatorial Vestalia Terra plateau. Large-scale troughs and ridges have regionally affected the surface. Between $180°E and $270°E, these tectonic features are well developed and related to the south pole Veneneia impact (Saturnalia Fossae trough unit), elsewhere on the hemisphere they are rare and subdued (Saturnalia Fossae cratered unit). In these pre-Rheasilvia units we observed an unexpectedly high frequency of impact craters up to $10 km in diameter, whose formation could in part be related to the Rheasilvia basin-forming event. The Rheasilvia impact has potentially affected the northern hemisphere also with S-N small-scale lineations, but without covering it with an ejecta blanket. Post-Rheasilvia impact craters are small (<60 km in diameter) and show a wide range of degradation states due to impact gardening and mass wasting processes. Where fresh, they display an ejecta blanket, bright rays and slope movements on walls. In places, crater rims have dark material ejecta and some crater floors are covered by ponded material interpreted as impact melt.

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Section: Geologic Mapsupporting

confidence: 89%

Section: Datasets and Methodsmentioning

confidence: 99%

Section: This Issue)mentioning

confidence: 99%

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Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Ruesch

Hiesinger

Blewett

et al. 2014

Icarus

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“…Secondary craters are expected on Pluto and Charon as well (Bierhaus and Dones, 2015), although of course they are generally much smaller than the primary craters that cause them. A general rule of thumb is that the largest secondaries are 0.05 the size of a given primary (Melosh, 1989), which is in line with more recent studies of icy satellite secondaries (Bierhaus et al, 2012;Singer et al, 2013). Although the largest, proximal secondaries on icy satellites can reach 0.1 the size of their generative primary, the sizes of distant secondaries, which are the ones that can be confused with the primary population (McEwen and Bierhaus, 2006), are much smaller.…”

Section: Secondary Craterssupporting

confidence: 57%

Impact and cratering rates onto Pluto

Greenstreet

Gladman

McKinnon³

2015

Icarus

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“…On the other hand, the icy and gas giants in the outer solar system have abundant small satellites that have low surface gravities, e.g., Enceladus (surface gravity ~ 0.113 m/ s 2 ) and Mimas (surface gravity ~ 0.064 m/s 2 ). Little or no traditional secondary craters should be formed on these bodies, because the minimum velocity required to form secondaries have exceeded the escape velocities of these bodies (Bierhaus et al 2012). However, most impact .…”

Section: Self-secondaries On the Other Planetary Bodiesmentioning

confidence: 99%

On the importance of self-secondaries

Xiao

2018

Geosci. Lett.

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Self-secondaries are secondary craters that are formed on both the continuous ejecta deposits and interior of the parent crater. The possible existence of self-secondaries was proposed in the late 1960s, but their identity, formation mechanism, and importance were not revisited until the new generation of high-resolution images for the Moon have recently became available. Possible self-secondary crater populations have now been recognized not only on the Moon, but also on Mercury, Mars, 1Ceres, 4Vesta, and satellites of the ice giants. On the Moon and terrestrial planets, fragments that form self-secondaries are launched with high ejection angles via spallation during the early cratering process, so that self-secondaries can be formed both within the crater and on the continuous ejecta deposits at the end of the cratering process. Self-secondaries potentially possess profound effects on the widely used agedetermination technique using crater statistics in planetary geology, because (1) self-secondaries cause nonuniform crater density across the continuous ejecta deposits, which cannot be solely explained by the effect of different target properties on crater size-frequency distributions; (2) crater chronologies for both the Moon and the other terrestrial bodies are largely based on crater counts on the continuous ejecta deposits of several young lunar craters. The effect of self-secondaries on crater chronology can be well addressed after the spatial distribution, size-frequency distribution, and density evolution of self-secondaries are resolved.

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The role of ejecta in the small crater populations on the mid-sized saturnian satellites

Cited by 53 publications

References 62 publications

Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Geologic map of the northern hemisphere of Vesta based on Dawn Framing Camera (FC) images

Impact and cratering rates onto Pluto

On the importance of self-secondaries

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